Progress in the Construction and Testing of the Tianlai Radio Interferometers
Santanu Das, Christopher J. Anderson, Reza Ansari, Jean-Eric Campagne, Daniel Charlet, Xuelei Chen, Zhiping Chen, Aleksander J. Cianciara, Pierre Colom, Yanping… 展开作者
Santanu Das, Christopher J. Anderson, Reza Ansari, Jean-Eric Campagne, Daniel Charlet, Xuelei Chen, Zhiping Chen, Aleksander J. Cianciara, Pierre Colom, Yanping Cong, Kevin G. Gayley, Jingchao Geng, Jie Hao, Qizhi Huang, Celeste S. Keith, Chao Li, Jixia Li, Yichao Li, Chao Liu, Tao Liu, Christophe Magneville, John P. Marriner, Jean-Michel Martin, Marc Moniez, Trevor M. Oxholm, Ue-Li Pen, Olivier Perdereau, Jeffrey B. Peterson, Huli Shi, Lin Shu, Albert Stebbins, Shijie Sun, Peter T. Timbie, Steve Torchinsky, Gregory S. Tucker, Guisong Wang, Rongli Wang, Xin Wang, Yougang Wang, Fengquan Wu, Yidong Xu, Kaifeng Yu, Jiao Zhang, Juyong Zhang, Le Zhang, Jialu Zhu, Shifan Zuo
天来探路者的设计是为了证明使用宽视场射电干涉仪来绘制再电离时代后宇宙中中性氢密度的可行性。这种称为21厘米强度测绘的方法，有望成为测量宇宙大尺度结构的廉价手段。天籁探路者目前由三个15米$\times$ 40米圆柱望远镜阵列和一个16个6米直径碟形天线阵列组成，位于中国西部无线电安静地区。选择这两种类型的阵列以确定每种方法的优点和缺点。探路者的主要目标是通过测量两个不同红移范围内的大面积天空$20,000 {\rm deg}^2$的中性氢来制作3D地图：首先是$1.03 > z > 0.78$（$700 - 800$ ~MHz），然后是$0.21 > z > 0.12$（$1170 - 1270$ ~MHz）。对$21$ ~cm强度测绘的最大挑战是去除使宇宙学信号相形见绌的强前景辐射。它需要对仪器响应的精确了解，即校准。在本文中，我们概述了探路者的现状，并讨论了我们为测量两个阵列的光束功能而进行的一些分析的细节。我们比较电磁模拟的阵列测量，讨论测量的增益和相稳定性的仪器，并提供了一个简要的概述的数据处理管道。
英文摘要：
The Tianlai Pathfinder is designed to demonstrate the feasibility of using a wide field of view radio interferometers to map the density of neutral hydrogen in the Universe after the Epoch of Reionizaton. This approach, called 21~cm intensity-mapping, promises an inexpensive means for surveying the large-scale structure of the cosmos. The Tianlai Pathfinder presently consists of an array of three, 15~m $\times$ 40~m cylinder telescopes and an array of sixteen, 6~m diameter dish antennas located in a radio-quiet part of western China. The two types of arrays were chosen to determine the advantages and disadvantages of each approach. The primary goal of the Pathfinder is to make 3D maps by surveying neutral hydrogen over large areas of the sky %$20,000 {\rm deg}^2$ in two different redshift ranges: first at $1.03 > z > 0.78$ ($700 - 800$~MHz) and later at $0.21 > z > 0.12$ ($1170 - 1270$~MHz). The most significant challenge to $21$~cm intensity-mapping is the removal of strong foreground radiation that dwarfs the cosmological signal. It requires exquisite knowledge of the instrumental response, i.e. calibration. In this paper, we provide an overview of the status of the Pathfinder and discuss the details of some of the analysis that we have carried out to measure the beam function of both arrays. We compare electromagnetic simulations of the arrays to measurements, discuss measurements of the gain and phase stability of the instrument, and provide a brief overview of the data processing pipeline.
Beamforming in Interferometer Arrays with Cross-couplings
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Science（中国科学院射电天文与技术重点实验室）；School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理学院）
Design and Commissioning of an LWA Swarm Station: The Long Wavelength Array -- North Arm
University of New Mexico（新墨西哥大学）；Air Force Research Laboratory, Space Vehicles Directorate（空军研究实验室空间飞行器管理局）；Curtin Institute of Radio Astronomy, Curtin University（科廷大学射电天文研究所）；United States Naval Observatory（美国海军天文台）；Hillsdale College（希尔斯代尔学院）
